Published October 31, 2024 | Version v1
Conference proceeding Open

Determining magnesium and silicon abundances from CARMENES spectra

Authors/Creators

  • 1. ROR icon Universidad Complutense de Madrid
  • 2. Centre for Planetary Habitability (University of Oslo)
  • 3. ROR icon Centro de Astrobiología
  • 4. Instituto de Astrofísica de Canarias
  • 5. Hamburger Sternwarte
  • 6. Max Planck Institute für Astronomie

Description

The study of chemical abundances of stars that host planets is critical to our current understanding of the structure, formation, evolution of rocky planets, and to understand the evolution and assembly of the Milky Way. Here we present the abundances of magnesium (Mg) and silicon (Si) for 314 dwarf stars with spectral types in the range K7.0-M5.5 observed using the high-resolution CARMENES spectrograph. Our spectroscopic analysis employs the BT-Settl model atmospheres, the radiative transfer code Turbospectrum, and a state-of-the-art selection of atomic and molecular data. The derived chemical abundances have a line-to-line scatter at the level of 0.1 dex for all studied spectral types, which is unprecedented at the latest sub-types. Based on the comparison of the results obtained for stellar components of multiple systems, we find that the total error bar for these abundances is at the level of 0.2 dex. Our computed abundances are broadly consistent with the galactic evolution trends of earlier FGK-type stars in the solar neighbourhood. Finally, we also explore the relation of the Mg and Si abundances of stars with and without known exoplanets.

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Additional details

Funding

Agencia Estatal de Investigación
Enanas frías como anfitrionas de exoplanetas: parámetros estelares y actividad magnética PID2022-137241NB-C44
Agencia Estatal de Investigación
Caracterización de estrellas y planetas PID2022-137241NB-C42
Comunidad de Madrid
TECNOLOGÍAS AVANZADAS PARA LA EXPLORACIÓN DEL UNIVERSO Y SUS COMPONENTES PR47/21 TAU-CM